1921.] Dhikoti-Karanam of Sripati. 276 
This is roughly a correction for the true place (longitude) of 
the Sun, and therefore also of the Moon, for, being at the end 
of Amavasya or Purnima, their longitudes can only differ by 0 
or 180. 
If the result as corrected is within 1 naksatra of either 
Node of the Moon, we should then proceed to the further 
consideration of an Eclipse, Lunar in ae case of a Purnima, 
and Solar in the case of Amavasya. Thus 1 naksatra on either 
side of the Node seems to be the jeer Eeliptic Limit. 
(4) Next to find the latitude of the Moon. ri difference 
of the result as obtained before, and 13"- ae 0°) or 
27"-0-0 (i.e., 360°) as the case may be, gives the Seccea dis- 
tance Prot the nearest Node. If the secult obtained in (3) is 
less than 13°-30%’-0, the latitude is North, but if it is greater 
than 13°-30°-0 and less than 27°-0-0, the latitude is South. 
Now the shortest distance just obtained measured in naksatras 
and naksatramsas (and of course less than 1 naksatra) gives 
the latitude if expressed in degrees, minutes and seconds. 
That is to say, 1 naksatra of longitude as measured from the 
Node corresponds to 1 degree of latitude. This is = elorree 
_to saying that the tangent of the inclination of the oon’s 
Orbit to the Ecliptic is about 3/40. This is why in ‘as first 
ibaa the difference in longitude was expressed in naksa- 
tramsa 
The latitude of the moon thus found is the latitude at 
the middle of the eclipse and at the end of the tithi (Amnavasye 
or Purnima). 
(5) In the case of the Lunar Eclipse the radius of the 
shadow at the distance of aed lunar orbit is taken to be 0-38’-0" 
and that of the Moon 0-1 
(a) Deducting from the sum 0- 56’-0” the latitude found 
in (4), we get the length of the of tion cut off. 
this is greater than 0-36’-0" the diameter of the 
Moon, there will be a Total Fires Eclipse. If the 
latitude is greater than 0-56’-0", there will be no 
e 
(b) The ane travelled by the Moon relative to the 
Sun from the commencement of the Eclipse to the 
Middle of the Eclipse is equal to the square root 
of the difference of the squares of the sum (56’) of 
the radii of the sea and the Moon and of the 
Latitude of the Moo 
(c) The Moon travels 730’ in n 60 nadikas (dandas) relative 
to the Sun. Thus by Rule of Three we get half the 
duration of the Eclipse 
(d) If there is a Total Eclipse, the time from the com- 
mencement of the total eclipse to the middle of the 
eclipse is obtained from the distance travelled by 
